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We generate probabilistic predictions of the low-redshift ($z < 0.2$)synchrotron Cosmic Web for half of the Northern Sky. In particular, we predictthe contribution to the specific intensity function at $\nu_\mathrm{obs} = 150\\mathrm{MHz}$ from merger shocks in clusters and accretion shocks in filaments,both of which arise during large-scale structure formation. We assume aprimordial magnetogenesis scenario, but our method is general enough to allowfor an exploration of alternative magnetogenesis scenarios - and evenalternative radiation mechanisms and spectral windows. In the future, bycomparing different predictions, one could infer the most plausible physicalmodel from a synchrotron Cosmic Web detection. Our method combines Bayesianlarge-scale structure reconstructions, snapshots of an MHD cosmologicalsimulation, a Gaussian random field, and a ray tracing approach. The resultshelp to select targets for deep observations and can be used in actualdetection experiments. We highlight predictions for the Hercules Cluster, theComa Cluster, Abell 2199, Abell 2255, the Lockman Hole and the Ursa MajorSupercluster. At degree-scale resolution, the median specific intensity reaches$m_{I_\nu} \sim 10^{-1}\ \xi_e\ \mathrm{Jy\ deg^{-2}}$, where $\xi_e$ is theelectron acceleration efficiency.

Filamentary Baryons and Where to Find Them: A forecast of synchrotron radiation from merger and accretion shocks in the local Cosmic Web